Studying Black-hole kicks BH-LMXB The Stars for All Meeting - - PowerPoint PPT Presentation

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Studying Black-hole kicks BH-LMXB The Stars for All Meeting - - PowerPoint PPT Presentation

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BH kicks S. Repetto Issue Studying Black-hole kicks BH-LMXB The Stars for All Meeting observed pop. Supernova kicks Serena Repetto 1 , 2 , Melvyn B. Davies 1 and S. Sigurdsson 3 Galactic orbits BPS, How 1 Lund Observatory to 2 Dept. of

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BH kicks

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BPS, How to BPS, results Single Sources Physics of the NK Conclusions

Studying Black-hole kicks

Stars for All Meeting Serena Repetto1,2, Melvyn B. Davies1 and S. Sigurdsson3

1Lund Observatory

  • 2Dept. of Astrophysics, Nijmegen
  • 3Dept. of Astronomy & Astrophysics, Pennsylvania State University

Lund, 7th February 2012

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Lund Observatory Master Thesis "Investigating Black-hole kicks" Melvyn B. Davies About to submit in MNRAS

  • Dept. of Astrophysics, Nijmegen

PhD student Gijs Nelemans, Peter Jonker

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BH kicks

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Do BHs receive kicks at birth?

Neutron stars get Natal Kicks at birth → 200 − 400 km/s from proper motion

Lyne & Lorimer 1994

Issue: Supernova → Mass Loss Kick (+ Natal Kick) What about stellar BHs? Same size as NS kicks? Best candidates: Black-holes in Low Mass X-ray Binaries BH+sun-like companion For free: Insights into how black-holes are formed!

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Previous Work

Willems et al. 2005 Gualandris et al. 2005 Fragos et al. 2009 Miller-Jones et al. 2009

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Black-holes in LMXBs

(a) BH binary orbit in the Galaxy for

107 − 109 (Rodrigues & Mirabel)

(b) Binary is now powered

by RLO (X-ray disk), artist impression.

Why: The supernova kicks the binary away from its planar o Which kick does it need in order to get to the current position? How: Synthetic population of BH-LMXBs

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Observed Galactic distribution

How do they get there?

High z (z > 1) or closer in (R 4), the trickiest NSs and BHs evidently similar...

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Observed Galactic distribution

How do they get there?

High z (z > 1) or closer in (R 4), the trickiest NSs and BHs evidently similar...

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Kicks of surviving binaries

Binary Kick: The supernova "kicks" the BH and its companion Sym SN Mass Loss Kick The binary recoils Binary Kick ∼ tens km/s Asym SN Mass Loss Kick+Natal Kick The NS recoils with VNK Binary Kick ∼ hundreds km/s What about BH? Full kick scenario: BH recoils with VNK Reduced kick scenario: The BH recoils with VNK × MNS MBH

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Modelling NS Natal Kicks

Hansen & Phinney 1997, one pick maxwellian Arzoumanian 2002, two peaks maxwellian Reduced kicks typically lower than 100 km/s

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Orbits in the Galaxy

Binary kick ∼ Galactic rotation → Dynamics changes The binary orbits in the Galaxy up to the present day LMXBs are typically old, 107-109 years Binary can move significantly from the plane! Necessary velocity: A simple argument...

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Orbits in the Galaxy

Maximum z reached by the binary for an optimal binary kick Some require binary kiks greater than 100 km/s Reduced kicks not enough? Typical Binary Kicks H&P : 230 km/s Bim: 200 km/s MCK-H&P 50 km/s MCK-Bim 60 km/s

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BH kicks

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BPS, How to

We populate the thin disk assuming SFR ∼ BFR We build a synthetic population of BH binaries taking average binary properties We impart the binary a Mass Loss Kick We impart the BH a Natal Kick drawn from different distribution (both full and reduced) Binary kick + Galactic rotation → Integration of trajectories for 109 years Galactic distribution of the synthetic pop.

  • Cf. Observed distribution → Fine tuning of the Natal

Kick

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BPS, results 1)

A zero Natal Kick (i.e. Mass Loss Kick alone) evidently fails!

2 4 6 8 10 12

  • 2

2

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BPS, results 1)

Full Natal Kicks appear to fit Reduced Natal Kicks give binaries more concentrated towards the plane

2 4 6 8 10

  • 2

2 2 4 6 8 10 12 R (kpc)

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BPS, results 2)

Black-hole Kick distribution

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Single sources

Three binaries show strong evidence for a the requirement of a full Natal Kick Name V⊥ VNK R z

(km/s) (km/s) (kpc) (kpc)

4U1543-47 95 80 3.92 0.70 1659-487 113

  • 3.25
  • 0.67

1819.3-2525 160 190 2.14

  • 0.82

XTEJ1118+480 80 70 8.73 1.50 1705-250 420 450 0.55 1.36 XTEJ1859+226 80

  • 7.23

1.20

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The physics of the (NS) Natal Kick

What is the propeller?

Hydrodynamically driven Convective instabilities Overstable oscillation of the progenitor core Neutrino driven (Lai et al. 2001) Black Holes are formed via: Prompt Collapse → No Natal Kick Fall back onto the proto-NS → Momentum Conserving Kick Other? Exotic? Accretion from companion Coalescence of a double-NS binary formed via fragmentation in the core-collapse (Davies et al. 2002)

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BH kicks

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Issue BH-LMXB The

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pop. Supernova kicks Galactic

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BPS, How to BPS, results Single Sources Physics of the NK Conclusions

The physics of the (NS) Natal Kick

What is the propeller?

Hydrodynamically driven Convective instabilities Overstable oscillation of the progenitor core Neutrino driven (Lai et al. 2001) Black Holes are formed via: Prompt Collapse → No Natal Kick Fall back onto the proto-NS → Momentum Conserving Kick Other? Exotic? Accretion from companion Coalescence of a double-NS binary formed via fragmentation in the core-collapse (Davies et al. 2002)

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Conclusions

We considered the pop. of BH-LMXBs as a function of the distribution of the Natal Kick Population: Full Natal Kicks make computed distribution more similar to observed Single Sources: Some strong candidates for full Natal Kicks

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Thank You!